This document summarizes Yuichi Otsuka's research on airglow observations and plasma bubbles in Indonesia. It discusses (1) airglow imaging from stations in Indonesia and Japan to study gravity waves and plasma bubbles, (2) the mechanism by which plasma bubbles form via the Rayleigh-Taylor instability exacerbated by prereversal electric fields, and (3) remaining uncertainties about the day-to-day drivers of plasma bubble occurrence.
Ionospheric TEC Disturbances over South KoreaFollowing the 2011 Great Tohoku ...researchinventy
Ionospheric total electron contents (TEC) disturbances following the 2011 great Tohoku earthquake on March 11, 2011 were observed by a GPS network in South Korea. The impulsive TEC enhancements were first observed approximately 16.5 minutes after the beginning of the earthquake. Various types of seismic waves were also observed over South Korea.To investigate more detailed disturbances in the TEC, we processed the GPS data with a sampling rate of 1Hz and applied a band-pass filter with corner frequencies of 0.0 and 0.005 Hz. Small-scale traveling ionospheric disturbances (TIDs) with a period of approximately 4minutes (~250 seconds) were observed from 6:15 to 7:10 UT. These variations are considered to be a clear manifestation of the acoustic resonance oscillations. We also observed medium-scale TIDs with a period of approximately 15 minutes and a duration of approximately 60 minutes. A remarkable finding is that the damping of the amplitude of the medium-scale TIDs was observed clearly in the time series
Discrete and broadband electron acceleration in Jupiter’s powerful auroraSérgio Sacani
The most intense auroral emissions from Earth’s polar regions,
called discrete for their sharply defined spatial configurations, are
generated by a process involving coherent acceleration of electrons
by slowly evolving, powerful electric fields directed along the
magnetic field lines that connect Earth’s space environment to its
polar regions1,2. In contrast, Earth’s less intense auroras are generally
caused by wave scattering of magnetically trapped populations of
hot electrons (in the case of diffuse aurora) or by the turbulent or
stochastic downward acceleration of electrons along magnetic field
lines by waves during transitory periods (in the case of broadband
or Alfvénic aurora)3,4. Jupiter’s relatively steady main aurora has a
power density that is so much larger than Earth’s that it has been
taken for granted that it must be generated primarily by the discrete
auroral process5–7. However, preliminary in situ measurements of
Jupiter’s auroral regions yielded no evidence of such a process8–10.
Here we report observations of distinct, high-energy, downward,
discrete electron acceleration in Jupiter’s auroral polar regions. We
also infer upward magnetic-field-aligned electric potentials of up to
400 kiloelectronvolts, an order of magnitude larger than the largest
potentials observed at Earth11. Despite the magnitude of these
upward electric potentials and the expectations from observations
at Earth, the downward energy flux from discrete acceleration is less
at Jupiter than that caused by broadband or stochastic processes,
with broadband and stochastic characteristics that are substantially
different from those at Earth.
X-RAY MEASUREMENTS OF THE PARTICLE ACCELERATION PROPERTIES AT INWARD SHOCKS I...Sérgio Sacani
We present new evidence that the bright non-thermal X-ray emission features in the interior of the Cassiopeia A
supernova remnant (SNR) are caused by inward moving shocks based on Chandra and NuSTAR observations. Several
bright inward-moving filaments were identified using monitoring data taken by Chandra in 2000–2014. These inwardmoving shock locations are nearly coincident with hard X-ray (15–40 keV) hot spots seen by NuSTAR. From proper
motion measurements, the transverse velocities were estimated to be in the range ∼2,100–3,800 km s−1
for a distance of
3.4 kpc. The shock velocities in the frame of the expanding ejecta reach values of ∼5,100–8,700 km s−1
, slightly higher
than the typical speed of the forward shock. Additionally, we find flux variations (both increasing and decreasing) on
timescales of a few years in some of the inward-moving shock filaments. The rapid variability timescales are consistent
with an amplified magnetic field of B ∼ 0.5–1 mG. The high speed and low photon cut-off energy of the inward-moving
shocks are shown to imply a particle diffusion coefficient that departs from the Bohm regime (k0 = D0/D0,Bohm ∼ 3–8)
for the few simple physical configurations we consider in this study. The maximum electron energy at these shocks is
estimated to be ∼8–11 TeV, smaller than the values of ∼15–34 TeV inferred for the forward shock. Cassiopeia A is
dynamically too young for its reverse shock to appear to be moving inward in the observer frame. We propose instead
that the inward-moving shocks are a consequence of the forward shock encountering a density jump of & 5–8 in the
surrounding material.
Ionospheric TEC Disturbances over South KoreaFollowing the 2011 Great Tohoku ...researchinventy
Ionospheric total electron contents (TEC) disturbances following the 2011 great Tohoku earthquake on March 11, 2011 were observed by a GPS network in South Korea. The impulsive TEC enhancements were first observed approximately 16.5 minutes after the beginning of the earthquake. Various types of seismic waves were also observed over South Korea.To investigate more detailed disturbances in the TEC, we processed the GPS data with a sampling rate of 1Hz and applied a band-pass filter with corner frequencies of 0.0 and 0.005 Hz. Small-scale traveling ionospheric disturbances (TIDs) with a period of approximately 4minutes (~250 seconds) were observed from 6:15 to 7:10 UT. These variations are considered to be a clear manifestation of the acoustic resonance oscillations. We also observed medium-scale TIDs with a period of approximately 15 minutes and a duration of approximately 60 minutes. A remarkable finding is that the damping of the amplitude of the medium-scale TIDs was observed clearly in the time series
Discrete and broadband electron acceleration in Jupiter’s powerful auroraSérgio Sacani
The most intense auroral emissions from Earth’s polar regions,
called discrete for their sharply defined spatial configurations, are
generated by a process involving coherent acceleration of electrons
by slowly evolving, powerful electric fields directed along the
magnetic field lines that connect Earth’s space environment to its
polar regions1,2. In contrast, Earth’s less intense auroras are generally
caused by wave scattering of magnetically trapped populations of
hot electrons (in the case of diffuse aurora) or by the turbulent or
stochastic downward acceleration of electrons along magnetic field
lines by waves during transitory periods (in the case of broadband
or Alfvénic aurora)3,4. Jupiter’s relatively steady main aurora has a
power density that is so much larger than Earth’s that it has been
taken for granted that it must be generated primarily by the discrete
auroral process5–7. However, preliminary in situ measurements of
Jupiter’s auroral regions yielded no evidence of such a process8–10.
Here we report observations of distinct, high-energy, downward,
discrete electron acceleration in Jupiter’s auroral polar regions. We
also infer upward magnetic-field-aligned electric potentials of up to
400 kiloelectronvolts, an order of magnitude larger than the largest
potentials observed at Earth11. Despite the magnitude of these
upward electric potentials and the expectations from observations
at Earth, the downward energy flux from discrete acceleration is less
at Jupiter than that caused by broadband or stochastic processes,
with broadband and stochastic characteristics that are substantially
different from those at Earth.
X-RAY MEASUREMENTS OF THE PARTICLE ACCELERATION PROPERTIES AT INWARD SHOCKS I...Sérgio Sacani
We present new evidence that the bright non-thermal X-ray emission features in the interior of the Cassiopeia A
supernova remnant (SNR) are caused by inward moving shocks based on Chandra and NuSTAR observations. Several
bright inward-moving filaments were identified using monitoring data taken by Chandra in 2000–2014. These inwardmoving shock locations are nearly coincident with hard X-ray (15–40 keV) hot spots seen by NuSTAR. From proper
motion measurements, the transverse velocities were estimated to be in the range ∼2,100–3,800 km s−1
for a distance of
3.4 kpc. The shock velocities in the frame of the expanding ejecta reach values of ∼5,100–8,700 km s−1
, slightly higher
than the typical speed of the forward shock. Additionally, we find flux variations (both increasing and decreasing) on
timescales of a few years in some of the inward-moving shock filaments. The rapid variability timescales are consistent
with an amplified magnetic field of B ∼ 0.5–1 mG. The high speed and low photon cut-off energy of the inward-moving
shocks are shown to imply a particle diffusion coefficient that departs from the Bohm regime (k0 = D0/D0,Bohm ∼ 3–8)
for the few simple physical configurations we consider in this study. The maximum electron energy at these shocks is
estimated to be ∼8–11 TeV, smaller than the values of ∼15–34 TeV inferred for the forward shock. Cassiopeia A is
dynamically too young for its reverse shock to appear to be moving inward in the observer frame. We propose instead
that the inward-moving shocks are a consequence of the forward shock encountering a density jump of & 5–8 in the
surrounding material.
Electromagnetic Phenomena Related to the 2011 Tohoku Earthquake and Tsunami: A Short Review by Stelios M Potirakis, Alexander Schekotov and Masashi Hayakawa in Examines in Marine Biology and Oceanography
NRT polarimetry and neutron star mergers - Nam 2019Joseph Fernandez
Talk given in the National Astronomy Meeting 2019, Lancaster, UK.
A large number of neutron star mergers will be detected by LIGO/Virgo in the coming years. GW170817 confirmed that neutron star mergers would actually produce relativistic outflows (e.g. relativistic jets and cocoon). The polarimetry by LT and NRT would enable us to study the properties of the outflow in details (i.e. magnetic field structure/strength, and its angular dependence). We discuss polarization signals in the outflow emission, and we show the expected signal distributions for an upcoming neutron star merger sample.
The experimental set up is enclosed in a highly evacuated glass vessel to avoid the deflection of silver atoms by gas. Each silver atom behaves like a magnet due to its magnetic moment resulting from spin angular momentum of its 5s1 electron. A beam of Silver atoms is passed in an inhomogeneous magnetic field. The silver atoms gets deflected in the inhomogeneous magnetic field due to the unequal forces experienced by poles of each 5s1 electron of an atom and is traced in a photographic plate. The presence of two curves on photographic film confirms that electron have spins either in clockwise or anticlockwise direction. The magnitude of the spacing between the curves on photographic film agrees well with experimental result. Thus, this experiment proves that space and spin of an electron is quantised and validates vector atom model.
Multi dimensional simulations_of_the_expanding_supernova_remnant_of_sn1987_aSérgio Sacani
Artigo descreve as mais novas simulações computacionais realizadas para se poder entender o funcionamento e a origem da remanescente de supernova SN1987A.
UNDERSTANDING WHAT GREEN WASHING IS!.pdfJulietMogola
Many companies today use green washing to lure the public into thinking they are conserving the environment but in real sense they are doing more harm. There have been such several cases from very big companies here in Kenya and also globally. This ranges from various sectors from manufacturing and goes to consumer products. Educating people on greenwashing will enable people to make better choices based on their analysis and not on what they see on marketing sites.
Electromagnetic Phenomena Related to the 2011 Tohoku Earthquake and Tsunami: A Short Review by Stelios M Potirakis, Alexander Schekotov and Masashi Hayakawa in Examines in Marine Biology and Oceanography
NRT polarimetry and neutron star mergers - Nam 2019Joseph Fernandez
Talk given in the National Astronomy Meeting 2019, Lancaster, UK.
A large number of neutron star mergers will be detected by LIGO/Virgo in the coming years. GW170817 confirmed that neutron star mergers would actually produce relativistic outflows (e.g. relativistic jets and cocoon). The polarimetry by LT and NRT would enable us to study the properties of the outflow in details (i.e. magnetic field structure/strength, and its angular dependence). We discuss polarization signals in the outflow emission, and we show the expected signal distributions for an upcoming neutron star merger sample.
The experimental set up is enclosed in a highly evacuated glass vessel to avoid the deflection of silver atoms by gas. Each silver atom behaves like a magnet due to its magnetic moment resulting from spin angular momentum of its 5s1 electron. A beam of Silver atoms is passed in an inhomogeneous magnetic field. The silver atoms gets deflected in the inhomogeneous magnetic field due to the unequal forces experienced by poles of each 5s1 electron of an atom and is traced in a photographic plate. The presence of two curves on photographic film confirms that electron have spins either in clockwise or anticlockwise direction. The magnitude of the spacing between the curves on photographic film agrees well with experimental result. Thus, this experiment proves that space and spin of an electron is quantised and validates vector atom model.
Multi dimensional simulations_of_the_expanding_supernova_remnant_of_sn1987_aSérgio Sacani
Artigo descreve as mais novas simulações computacionais realizadas para se poder entender o funcionamento e a origem da remanescente de supernova SN1987A.
UNDERSTANDING WHAT GREEN WASHING IS!.pdfJulietMogola
Many companies today use green washing to lure the public into thinking they are conserving the environment but in real sense they are doing more harm. There have been such several cases from very big companies here in Kenya and also globally. This ranges from various sectors from manufacturing and goes to consumer products. Educating people on greenwashing will enable people to make better choices based on their analysis and not on what they see on marketing sites.
Willie Nelson Net Worth: A Journey Through Music, Movies, and Business Venturesgreendigital
Willie Nelson is a name that resonates within the world of music and entertainment. Known for his unique voice, and masterful guitar skills. and an extraordinary career spanning several decades. Nelson has become a legend in the country music scene. But, his influence extends far beyond the realm of music. with ventures in acting, writing, activism, and business. This comprehensive article delves into Willie Nelson net worth. exploring the various facets of his career that have contributed to his large fortune.
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Introduction
Willie Nelson net worth is a testament to his enduring influence and success in many fields. Born on April 29, 1933, in Abbott, Texas. Nelson's journey from a humble beginning to becoming one of the most iconic figures in American music is nothing short of inspirational. His net worth, which estimated to be around $25 million as of 2024. reflects a career that is as diverse as it is prolific.
Early Life and Musical Beginnings
Humble Origins
Willie Hugh Nelson was born during the Great Depression. a time of significant economic hardship in the United States. Raised by his grandparents. Nelson found solace and inspiration in music from an early age. His grandmother taught him to play the guitar. setting the stage for what would become an illustrious career.
First Steps in Music
Nelson's initial foray into the music industry was fraught with challenges. He moved to Nashville, Tennessee, to pursue his dreams, but success did not come . Working as a songwriter, Nelson penned hits for other artists. which helped him gain a foothold in the competitive music scene. His songwriting skills contributed to his early earnings. laying the foundation for his net worth.
Rise to Stardom
Breakthrough Albums
The 1970s marked a turning point in Willie Nelson's career. His albums "Shotgun Willie" (1973), "Red Headed Stranger" (1975). and "Stardust" (1978) received critical acclaim and commercial success. These albums not only solidified his position in the country music genre. but also introduced his music to a broader audience. The success of these albums played a crucial role in boosting Willie Nelson net worth.
Iconic Songs
Willie Nelson net worth is also attributed to his extensive catalog of hit songs. Tracks like "Blue Eyes Crying in the Rain," "On the Road Again," and "Always on My Mind" have become timeless classics. These songs have not only earned Nelson large royalties but have also ensured his continued relevance in the music industry.
Acting and Film Career
Hollywood Ventures
In addition to his music career, Willie Nelson has also made a mark in Hollywood. His distinctive personality and on-screen presence have landed him roles in several films and television shows. Notable appearances include roles in "The Electric Horseman" (1979), "Honeysuckle Rose" (1980), and "Barbarosa" (1982). These acting gigs have added a significant amount to Willie Nelson net worth.
Television Appearances
Nelson's char
WRI’s brand new “Food Service Playbook for Promoting Sustainable Food Choices” gives food service operators the very latest strategies for creating dining environments that empower consumers to choose sustainable, plant-rich dishes. This research builds off our first guide for food service, now with industry experience and insights from nearly 350 academic trials.
"Understanding the Carbon Cycle: Processes, Human Impacts, and Strategies for...MMariSelvam4
The carbon cycle is a critical component of Earth's environmental system, governing the movement and transformation of carbon through various reservoirs, including the atmosphere, oceans, soil, and living organisms. This complex cycle involves several key processes such as photosynthesis, respiration, decomposition, and carbon sequestration, each contributing to the regulation of carbon levels on the planet.
Human activities, particularly fossil fuel combustion and deforestation, have significantly altered the natural carbon cycle, leading to increased atmospheric carbon dioxide concentrations and driving climate change. Understanding the intricacies of the carbon cycle is essential for assessing the impacts of these changes and developing effective mitigation strategies.
By studying the carbon cycle, scientists can identify carbon sources and sinks, measure carbon fluxes, and predict future trends. This knowledge is crucial for crafting policies aimed at reducing carbon emissions, enhancing carbon storage, and promoting sustainable practices. The carbon cycle's interplay with climate systems, ecosystems, and human activities underscores its importance in maintaining a stable and healthy planet.
In-depth exploration of the carbon cycle reveals the delicate balance required to sustain life and the urgent need to address anthropogenic influences. Through research, education, and policy, we can work towards restoring equilibrium in the carbon cycle and ensuring a sustainable future for generations to come.
Characterization and the Kinetics of drying at the drying oven and with micro...Open Access Research Paper
The objective of this work is to contribute to valorization de Nephelium lappaceum by the characterization of kinetics of drying of seeds of Nephelium lappaceum. The seeds were dehydrated until a constant mass respectively in a drying oven and a microwawe oven. The temperatures and the powers of drying are respectively: 50, 60 and 70°C and 140, 280 and 420 W. The results show that the curves of drying of seeds of Nephelium lappaceum do not present a phase of constant kinetics. The coefficients of diffusion vary between 2.09.10-8 to 2.98. 10-8m-2/s in the interval of 50°C at 70°C and between 4.83×10-07 at 9.04×10-07 m-8/s for the powers going of 140 W with 420 W the relation between Arrhenius and a value of energy of activation of 16.49 kJ. mol-1 expressed the effect of the temperature on effective diffusivity.
Natural farming @ Dr. Siddhartha S. Jena.pptxsidjena70
A brief about organic farming/ Natural farming/ Zero budget natural farming/ Subash Palekar Natural farming which keeps us and environment safe and healthy. Next gen Agricultural practices of chemical free farming.
16. 120 m/s
Zonal drift velocity of F-region
FAI (plasma bubble) is consistent
with zonal component of the
thermospheric neutral wind over
Kototabang.
F-region FAI Observed
With EAR
Local Time
Longitude
South
East
plasma bubble motion ⇔ ExB drift
E-field is generated mainly by neutral wind over
20. GPS Scintillation （Indonesia）
2003 2004 2005 2006 2007
J
F
M
A
M
J
J
A
S
O
N
D
19 0 619 0 6 19 0 6 19 0 6
19 0 6
Local Time (hours)
S4
GPS scintillation occurs between
sunset and midnight in equinox.
Occurrence rate decreases with
decrease of solar activity.
25. growth rate ： g
Growth Rate of the Rayleigh-Taylor Instability
Eastward E is effective because
- contribute to eastward J.
- move the F-region plasma to higher altitude. At high altitude,
gxB current become effective.
E: eastward electric field
B: magnetic field
b: gravitational acceleration
nin : collision frequency
n: plasma density
z: altitude
26. Vertical Drift
（positive upward）
= Eastward Electric Field
At the evening terminator,
drift velocity upward → downward
electric field eastward → westward
(evening enhancement;
pre-reversal enhancement)
27. Mechanism Generating Evening Enhancement
[Farley et al., 1986]
U
Ez= -UxB
Hall J
Map to E-region
Electric
Field
Negative Charge
Map to F-region
Upward
ExB
→ bubble
28. GPS Scintillation （Indonesia）
2003 2004 2005 2006 2007
J
F
M
A
M
J
J
A
S
O
N
D
19 0 619 0 6 19 0 6 19 0 6
19 0 6
Local Time (hours)
S4
GPS scintillation occurs between
sunset and midnight in equinox.
Occurrence rate decreases with
decrease of solar activity.
30. Plasma Bubble Occurrence
• Seasonal and longitudinal variation is well
understood and can be explained by the pre-reversal
enhancement.
• For the purpose of the space weather, we need to
know where and when plasma bubbles occur.
• Mechanism of the day-to-day variation is unknown.
There are 3 candidate:
1. Upward propagating GW
2. LSWS (Large-Scale Wave Structure)
3. Meridional Neutral Wind
(asymmetry of equatorial anomaly)
No conclusive evidence showing which mechanisms are most effective.
